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@ARTICLE{Hanauske:208887,
      author       = {Hanauske, Matthias and Takami, Kentaro and Bovard, Luke and
                      Rezzolla, Luciano and Font, José A. and Galeazzi, Filippo
                      and Stöcker, Horst},
      title        = {{R}otational properties of hypermassive neutron stars from
                      binary mergers},
      journal      = {Physical review / D},
      volume       = {96},
      number       = {4},
      issn         = {2470-0010},
      address      = {Woodbury, NY},
      publisher    = {Inst.},
      reportid     = {GSI-2018-00269, arXiv:1611.07152},
      pages        = {043004},
      year         = {2017},
      note         = {*Brief entry*25 pages, 20 figures},
      abstract     = {Determining the differential-rotation law of compact
                      stellar objects produced in binary neutron stars mergers or
                      core-collapse supernovae is an old problem in relativistic
                      astrophysics. Addressing this problem is important because
                      it impacts directly on the maximum mass these objects can
                      attain and, hence, on the threshold to black-hole formation
                      under realistic conditions. Using the results from a large
                      number of numerical simulations in full general relativity
                      of binary neutron star mergers described with various
                      equations of state and masses, we study the rotational
                      properties of the resulting hypermassive neutron stars. We
                      find that the angular-velocity distribution shows only a
                      modest dependence on the equation of state, thus exhibiting
                      the traits of “quasiuniversality” found in other aspects
                      of compact stars, both isolated and in binary systems. The
                      distributions are characterized by an almost uniformly
                      rotating core and a “disk.” Such a configuration is
                      significantly different from the j-constant
                      differential-rotation law that is commonly adopted in
                      equilibrium models of differentially rotating stars.
                      Furthermore, the rest-mass contained in such a disk can be
                      quite large, ranging from ≃0.03  M⊙ in the case of
                      high-mass binaries with stiff equations of state, up to
                      ≃0.2  M⊙ for low-mass binaries with soft equations
                      of state. We comment on the astrophysical implications of
                      our findings and on the long-term evolutionary scenarios
                      that can be conjectured on the basis of our simulations.},
      cin          = {THE},
      ddc          = {530},
      cid          = {I:(DE-Ds200)THE-20051214OR028},
      pnm          = {612 - Cosmic Matter in the Laboratory (POF3-612)},
      pid          = {G:(DE-HGF)POF3-612},
      typ          = {PUB:(DE-HGF)29 / PUB:(DE-HGF)16},
      eprint       = {1611.07152},
      howpublished = {arXiv:1611.07152},
      archivePrefix = {arXiv},
      SLACcitation = {$\%\%CITATION$ = $arXiv:1611.07152;\%\%$},
      UT           = {WOS:000407020400002},
      doi          = {10.1103/PhysRevD.96.043004},
      url          = {https://repository.gsi.de/record/208887},
}